Constraints on the Origin of Kepler's Supernova Remnant

Details Constraints on the Origin of Kepler's Supernova Remnant Constraints on the Origin of Kepler's Supernova Remnant

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.3303p&link_type=abstract

American Astronomical Society, HEAD meeting #12, #33.03

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Scientific paper

It is now well established that Kepler's supernova remnant (SNR) is the result of a Type Ia explosion. With an age of 407 yr, Kepler is estimated to be 3.5 to 7.5 kpc distant, with an angular diameter of 5 arcminutes. Unlike other Galactic Type Ia SNRs (e.g. Tycho's SNR and SN 1006), Kepler shows strong evidence for circumstellar interaction. A bowshock structure in the north of the SNR is thought to originate from the movement of the mass-losing progenitor through the interstellar medium prior to the supernova. We present results of a modeling campaign aimed at constraining the mass loss history of the progenitor and the amount of 56Ni synthesized in the explosion through hydrodynamic and NEI calculations of the SNR evolution. We simulate the interaction of realistic SN Ia ejecta models with circumstellar density profiles sculpted by mass loss from several SN Ia progenitor scenarios and compare the results to the bulk properties of the X-ray emission and SNR dynamics.

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